The K spectral type contact binary NSVS 1557555: Photometric solution and preliminary elements

Barani, C.; Acerbi, Francesco; Martignoni, M.

doi:10.1016/j.newast.2017.06.006

Cited by 3 publications

(2 citation statements)

References 33 publications

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“…The first system in our sample is V1297 Cas (= HD 232102 = NSVS 1557555), which is also the one with the latest spectral type classification (K0 according to Cannon 1927). It was quite recently studied photometrically, when Barani et al (2017) published their BV I c light curves. Their detailed analysis revealed that this W UMa-type contact binary with an orbital period of about 0.27 days has an inclination of about 85 • and mass ratio q = 0.55.…”

Section: V1297 Casmentioning

confidence: 99%

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Light-time effect detected in fourteen eclipsing binaries

Zasche

Uhlàř²,

Svoboda³

et al. 2020

A&A

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Cyg) were collected and analyzed. Using the automatic telescopes, surveys, and satellite data, we derived more than 2500 times of eclipses, accompanied with our own groundbased observations. These data were used to detect the period variations in these multiple systems. The eclipse timing variations (ETVs) were described using the third-body hypothesis and the light-time effect. Their respective periods were derived as 2.5, 16.2,

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Section: V1297 Casmentioning

confidence: 99%

“…This indicates that the third body should have at least M 3,min = 1.32 M ⊙ (assuming the coplanar orbits). On the other hand, Barani et al (2017) estimated the spectral type of the third body as G7. To conclude, we can certainly state that the third component is the dominant body in the system.…”

Section: V1297 Casmentioning

confidence: 99%

Light-time effect detected in fourteen eclipsing binaries

Zasche

Uhlàř²,

Svoboda³

et al. 2020

A&A

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Orbital period cut-off of W UMa-type contact binaries

Zhang

Qian

2020

Monthly Notices of the Royal Astronomical Society

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Period cut-off and period-color relation are two special characters of W UMa-type contact binaries. In the past, many authors noted these two properties, however, a comprehensive study was still lacking. In order to reveal a theoretical mechanism behind these two peculiarities, we collected 370 contact binaries whose orbital periods, mass ratios, masses and radii are compiled and attempted to make this idea come true by statistical means. Then, we obtained a lower limit (0.15 days) of orbital period by studying the correlation among four physical parameters (orbital period P, mass ratio q, mass of primary star M1 and separation between two components a). Furthermore, we used the most reliable parameters (P and q) to check our result, fortunately, all evidence indicated that our predicted value is credible. In the end, the reason why the period-color relation exist was also discussed.

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Investigation of the orbital period and mass relations for W UMa-type contact systems

Poro¹,

Sarabi²,

Zamanpour

et al. 2021

Monthly Notices of the Royal Astronomical Society

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New relationships between the orbital period and some parameters of W Ursae Majoris (W UMa) type systems are presented in this study. To investigate the relationships, we calculated the absolute parameters of a sample of 118 systems. For this purpose, we used the parallax values obtained from the Gaia Early Data Release 3 (Gaia EDR3) star catalog for more precise calculations. The other required parameters, including the light curve solutions and the orbital period were derived from previous research. For some relationships, we added 86 systems from another study with an orbital period of less than 0.6 days to our sample, allowing us to increase the number of systems to 204. Therefore, the mass (M) values of each component along with all the other absolute parameters were recalculated for these contact systems. We used the Markov Chain Monte Carlo (MCMC) approach in order to gain the new orbital period-mass relations (P − M) per component, and added the temperature (T) to the process to acquire the new orbital period-temperature (P − T1) relation. We presented the orbital period behaviour in terms of log(g) by new relations for each component. We have also obtained a model between the orbital period, the mass of the primary component and temperature (P − M1 − T1) using the Artificial Neural Networks (ANN) method. Additionally, we present a model for the relationship between the orbital period and the mass ratio (P − q) by fitting a Multi-Layer Perceptron (MLP) regression model to a sample of the data collected from the literature.

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The K spectral type contact binary NSVS 1557555: Photometric solution and preliminary elements

Cited by 3 publications

References 33 publications

Light-time effect detected in fourteen eclipsing binaries

Light-time effect detected in fourteen eclipsing binaries

Orbital period cut-off of W UMa-type contact binaries

Investigation of the orbital period and mass relations for W UMa-type contact systems

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